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A New Titan GCM and Stratospheric Superrotation Yuan Lian, Claire Newman, Mark Richardson and Chris Lee Work funded through the OPR program, and simulations performed on the NASA Ames High End Computing cluster

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Goals of this work To reproduce key aspects of Titan’s circulation in a 3-dimensional general circulation model (GCM) To form a robust understanding of the dynamical mechanisms responsible To produce robust predictions of seasonal changes in Titan’s circulation

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Pressure (mbar) CIRS zonal winds for L s ~ ° TitanWRF zonal winds for same period Zonal wind peaks at a lower altitude than observed (likely due to the ‘low’ model top and/or the lack of active haze advection) Discrepancies between TitanWRF and observations Also, no lower stratosphere zonal wind minimum as seen by Huygens and also Cassini (Flasar, 2012)

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Question 1: Does another GCM using identical radiative forcing produce a similar circulation? - This is actually a well-known problem in Titan modeling Question 2: Do we see episodic ‘transfer events’ in a different Titan GCM? - How robust is our proposed superrotation mechanism? Question 3: How delicate are the wave interactions involved in driving Titan’s equatorial superrotation? - Was the need to minimize mixing limited to TitanWRF? Questions we wanted to answer

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We examined two GCMs and four setups. Setups 1 & 2 used our first Titan GCM, TitanWRF… 1.TitanWRF [Newman et al., Icarus, 2011] Lat-lon grid, finite-difference solver 2.TitanWRF with a ‘rotated pole’ Numerical pole and ‘polar’ filtering now at the equator Filtering to avoid instabilities where grid spacing is small Grid rotated through 90°

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Which produced realistic superrotation? 1.TitanWRF with a standard lat-lon grid 2.Titan MITgcm with a standard lat-lon grid Which had problems? 2. TitanWRF with rotated pole4. MITgcm with cubed-sphere grid

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What do the problem set-ups have in common? In both cases, we’re ‘messing with’ the low- to mid- latitudes where the waves are produced that are crucial to driving superrotation TitanWRF with rotated pole Titan MITgcm with cubed-sphere grid Has filtered regions at both numerical poles Has 6 special ‘corner’ points

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Superrotation index for the MITgcm lat-lon grid Superrotation index = mass-weighted angular momentum of layer that of same layer at rest wrt the solid surface

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Question 3: How delicate are the wave interactions involved in driving Titan’s equatorial superrotation? - Was the need to minimize mixing limited to TitanWRF? Answer from this work: The dynamics of the low- to mid-latitudes should be treated very carefully to avoid disrupting vital wave-mean flow interactions - This does not seem to be limited to TitanWRF Questions we wanted to answer

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Question 2: Do we see episodic ‘transfer events’ in a different Titan GCM? - How robust is our proposed superrotation mechanism? Answer from this work: Momentum transport in the Titan MITgcm is remarkably close to that in TitanWRF despite big differences in dynamical core / numerics - The mechanism appears to be quite robust Questions we wanted to answer

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The circulation in TitanWRF and the MITgcm Comparing temperatures at L s = 270°: largely look very similar, but slight variations can have a big impact on dynamics Pressure (mbar) TitanWRF Titan MITgcm

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Question 1: Does another GCM using identical radiative forcing produce a similar circulation? - This is actually a well-known problem in Titan modeling Answer: Many similarities, but differences in detail: e.g. superrotation strength; sharper vertical gradients - Much more to investigate here! Questions we wanted to answer

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Conclusions At Ashima we now have two superrotating Titan GCMs with similarly realistic circulations: TitanWRF and Titan MITgcm Our proposed mechanism for the production of equatorial stratospheric superrotation in TitanWRF – via ‘episodic transfer events’ – is supported by Titan MITgcm results As found before, GCM set-ups that disrupt the low- to mid- latitudes (e.g. too much diffusion, filtering, etc.) disrupt the delicate wave momentum transports responsible Titan MITgcm also captures far more of the observed zonal wind minimum above the tropopause than TitanWRF – Could be due to improved accuracy of temperature advection – However, tropospheric wind speeds in Titan MITgcm are too small

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Future work Raise the model top for both models to cover more of the haze production zone Turn on radiatively active advection of haze particles to enable feedbacks between haze distribution, heating and circulation These changes should allow a stronger circulation to develop and reduce interference by the model top, thus improving the match to observations